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New neon-abundance results in Galactic WN and WC stars

Published online by Cambridge University Press:  26 May 2016

John-David T. Smith
John-David T. Smith*
Affiliation:
Steward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721, USA

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The fast, dense winds which characterize Wolf-Rayet stars obscure their underlying cores, and complicate the verification of evolving core and nucleosynthesis models. A powerful technique for probing WR core evolution involves measuring abundances of wind-borne nuclear processed elements. Neon, in particular, undergoes a remarkable change in abundance during the later stages of a WR star's lifetime. By the end of the WC phase, it becomes the fourth most abundant element, after He, C and O (Maeder 1983).

Type
Part 1. Atmospheres of Massive Stars
Information
Symposium - International Astronomical Union , Volume 212: A Massive Star Odyssey: From Main Sequence to Supernova , 2003 , pp. 234 - 235
Copyright
Copyright © Astronomical Society of the Pacific 2003 

References

Aitken, D.K., Roche, P.F., Allen, D.A. 1982, MNRAS (Letters) 200, 69P.CrossRefGoogle Scholar
Barlow, M.J., Roche, P.F., Aitken, D.K. 1988, MNRAS 232, 821.CrossRefGoogle Scholar
Dessart, L., Crowther, P.A., Hillier, D.J., Willis, A.J., Morris, P.W., van der Hucht, K.A. 2000, MNRAS 315, 407.Google Scholar
van der Hucht, K.A., Olnon, F.M. 1985, A&A (Letters) 149, L17.Google Scholar
Maeder, A. 1983, A&A 120, 113.Google Scholar
Smith, J.D.T., Houck, J.R. 2001, AJ 121, 2115.Google Scholar